Alfven Wave-Driven Supernova Explosion

Abstract

We investigate the role of Alfven waves in the core-collapse supernova (SN) explosion. We assume that Alfven waves are generated by convections inside a proto-neutron star (PNS) and emitted from its surface. Then these waves propagate outwards, dissipate via nonlinear processes, and heat up matter around a stalled prompt shock. To quantitatively assess the importance of this process for the revival of the stalled shock, we perform 1D time-dependent hydrodynamical simulations, taking into account the heating via the dissipation of Alfven waves that propagate radially outwards along open flux tubes. We show that the shock revival occurs if the surface field strength is larger than ~2e15 G and if the amplitude of velocity fluctuation at the PNS surface is larger than 20% of the local sound speed. Interestingly, the Alfven wave mechanism is self-regulating in the sense that the explosion energy is not very sensitive to the surface field strength and initial amplitude of Alfven waves as long as they are larger than the threshold values given above.

7 pages, 3 figures embedded, submitted to ApJ

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• Hydrodynamics of core-collapse supernovae and their progenitors
• Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae
• Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores
• Measuring the Angular Momentum Distribution in Core-Collapse Supernova Progenitors with Gravitational Waves
• Turbulent Magnetic Field Amplification from Spiral SASI Modes: Implications for Core-Collapse Supernovae and Proto-Neutron Star Magnetization
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• Revisiting Impacts of Nuclear Burning for Reviving Weak Shocks in Neutrino-Driven Supernovae
• Dynamics of an Alfven surface in core collapse supernovae
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• Toward a magnetohydrodynamic theory of the stationary accretion shock: toy model of the advective-acoustic cycle in a magnetized flow
• The Evolution of High Temperature Plasma in Magnetar Magnetospheres and its Implications for Giant Flares